5/29/25

 The variables identified in this study are listed in Table [tsr: Table doesn’t exist yet].35
A map of their positions, and an H-R diagram showing their colors and magnitudes, is shown in Figure(s) [tsr:36
Figures don’t exist yet].

5/28/25

 We identified variables using the following methods.21
1. the Stetson variability index (P. Stetson 1996);22
2. reduced chi-squared (χ2
ν );23
3. the Lomb-Scargle periodogram (N. R. Lomb 1976; J. D. Scargle 1982; J. T. VanderPlas 2018).24
Objects were identified as variable if they met any of the following three criteria:25
1. the ”automatic Stetson” criterion: its light curve was high signal-to-noise, free from major photometric processing26
error flags, and showed a Stetson index exceeding the 99.7th percentile (a ”three-sigma” equivalent) for its27
magnitude range;28
2. the ”periodic” criterion: the object was identified as a periodic variable;29
3. the ”subjective” criterion: the object was in neither of the above two groups, but had a χ2
ν in at least one30
band consistent with variability, and upon manual inspection, displayed a light curve which showed unambigu-31
ous correlated variability across multiple bands that was not purely stochastic and could not be produced by32
photometric processing errors or artifacts.

5/26/25

 We looked at the star forming regions NGC 1333 and IC 348 for 6+ months each. It was with UKIRT, using the WCFAM instrument, monitoring in J, H, and K. In our monitoring of 539 stellar
and substellar cluster members with spectral types from M0-L3, we have identified 265 variables,
including 143 periodic variables